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Determining the Daytime Earth Radiative Flux from National Institute of Standards and Technology Advanced Radiometer (NISTAR) Measurements” by Wenying Su Et Al

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Determining the Daytime Earth Radiative Flux from National Institute of Standards and Technology Advanced Radiometer (NISTAR) Measurements” by Wenying Su Et Al Generated using version 3.2 of the official AMS LATEX template 1 Determining the Daytime Earth Radiative Flux from National 2 Institute of Standards and Technology Advanced Radiometer 3 (NISTAR) Measurements 1 2 2 2 4 Wenying Su , Patrick Minnis , Lusheng Liang , David P. Duda , Konstantin Khlopenkov2, Mandana M. Thieman2, Yinan Yu3, Allan Smith3, Steven Lorentz3, Daniel Feldman4, Francisco P. J. Valero5 1Science Directorate, NASA Langley Research Center, Hampton, Virginia 2Science Systems & Applications, Inc., Hampton, Virginia 3L-1 Standards and Technology, Inc., New Windsor, Maryland 4Lawrence Berkeley National Laboratory, MS 84R0171, Berkeley, California 5Scripps Institute of Oceanography, University of California, San Diego, CA, USA 1 5 ABSTRACT 6 The National Institute of Standards and Technology Advanced Radiometer (NISTAR) on- 7 board Deep Space Climate Observatory (DSCOVR) provides continuous full disc global 8 broadband irradiance measurements over most of the sunlit side of the Earth. The three ac- 9 tive cavity radiometers measures the total radiant energy from the sun-lit side of the Earth in 10 shortwave (SW, 0.2-4 µm), total (0.4-100 µm), and near-infrared (NIR, 0.7-4 µm) channels. 11 The Level 1 NISTAR dataset provides the filtered radiances (the ratio between irradiance 12 and solid angle). To determine the daytime top-of-atmosphere (TOA) shortwave and long- 13 wave radiative fluxes, the NISTAR measured shortwave radiances must be unfiltered first. 14 An unfiltering algorithm was developed for the NISTAR SW and NIR channels using a spec- 15 tral radiance data base calculated for typical Earth scenes. The resulting unfiltered NISTAR 16 radiances are then converted to full disk daytime SW and LW flux, by accounting for the 17 anisotropic characteristics of the Earth-reflected and emitted radiances. The anisotropy fac- 18 tors are determined using scene identifications determined from multiple low Earth orbit and 19 geostationary satellites and the angular distribution models (ADMs) developed using data 20 collected by the Clouds and the Earth's Radiant Energy System (CERES). Global annual 21 daytime mean SW fluxes from NISTAR are about 6% greater than those from CERES, and 22 both show strong diurnal variations with daily maximum-minimum differences as great as −2 23 20 Wm depending on the conditions of the sunlit portion of the Earth. They are also 24 highly correlated, having correlation coefficients of 0.89, indicating that they both capture 25 the diurnal variation. Global annual daytime mean LW fluxes from NISTAR are 3% greater 26 than those from CERES, but the correlation between them is only about 0.38. 1 27 1. Introduction 28 The Earth's climate is determined by the amount and distribution of the incoming so- 29 lar radiation absorbed and the outgoing longwave radiation (OLR) emitted by the Earth. 30 Satellite observations of Earth Radiation Budget (ERB) provide critical information needed 31 to better understand the driving mechanisms of climate change; the ERB has been moni- 32 tored from space since the early satellite missions of the late 1950s and the 1960s (House 33 et al. 1986). Currently, the Clouds and the Earth's Radiant Energy System (CERES) in- 34 struments (Wielicki et al. 1996; Loeb et al. 2016) have been providing continuous global 35 top-of-atmosphere (TOA) reflected shortwave radiation and OLR since 2000. CERES data 36 have been crucial to advance our understanding of the Earth's energy balance (e.g., Tren- 37 berth et al. 2009; Kato et al. 2011; Loeb et al. 2012; Stephens et al. 2012), aerosol direct 38 radiative effects (e.g., Satheesh and Ramanathan 2000; Zhang et al. 2005; Loeb and Manalo- 39 Smith 2005; Su et al. 2013), aerosol-cloud interactions (e.g., Loeb and Schuster 2008; Quaas 40 et al. 2008; Su et al. 2010b), and to evaluate global general circulation models (e.g., Pincus 41 et al. 2008; Su et al. 2010a; Wang and Su 2013; Wild et al. 2013). 42 The Earth's radiative flux data record is augmented by the launch of the Deep Space 43 Climate Observatory (DSCOVR) on February 11, 2015. DSCOVR is designed to continu- 44 ously monitor the sunlit side of the Earth, being the first Earth-observing satellite at the 45 Lagrange-1 (L1) point, ∼1.5 million km from Earth, where it orbits the Sun at the same 46 rate as the Earth (see Figure 1a). DSCOVR is in an elliptical Lissajous orbit around the 47 L1 point and is not positioned exactly on the Earth-sun line, therefore only about 92∼97% 48 of the sunlit Earth is visible to DSCOVR. As illustrated in Figure 1b, the daytime portion 49 (Ah) is not visible to the DSCOVR. Strictly speaking, the measurements from DSCOVR 50 are not truly `global' daytime measurements. However, for simplicity we refer to them as 51 global daytime measurements. Onboard DSCOVR, the National Institute of Standards and 52 Technology Advanced Radiometer (NISTAR) provides continuous full disc global broadband 53 irradiance measurements over most of the sunlit side of the Earth (viewing the sunlit side 2 54 of the Earth as one pixel). Besides NISTAR, DSCOVR also carries the Earth Polychromatic 55 Imaging Camera (EPIC) which provides 2048 by 2048 pixel imagery 10 to 22 times per day 56 in 10 spectral bands from 317 to 780 nm. On June 8, 2015, more than 100 days after launch, 57 DSCOVR started orbiting around the L1 point. 58 The NISTAR instrument was designed to measure the global daytime shortwave (SW) 59 and longwave (LW) radiative fluxes. The original objective of NISTAR was to monitor 60 the energy from the sunlit side of the Earth continuously, and to understand the effects of 61 weather systems and clouds on the daytime energy. However, one limitation of NISTAR is 62 its relatively low signal-to-noise ratios, which necessitates averaging significant time periods 63 to adequately reduce the instrument noise levels. This constrains the temporal resolution 64 of meaningful results to about 4 hours, thus prevent us from \continuously" monitoring the 65 sunlit side of the Earth. Nevertheless, NISTAR measurements can still be useful for assessing 66 the hourly fluxes produced by combining the observations from multiple low-Earth orbit and 67 geostationary satellites (Doelling et al. 2013) and for model evaluation using the spectral 68 ratio information (Carlson et al. 2019). NISTAR measures an irradiance at the L1 point at ◦ ◦ 69 a small relative azimuth angle, φo, which varies from 4 to 15 , as shown in Figure 1a. As 70 such, the radiation it measures comes from the near-backscatter position, which is different 71 from that seen at other satellite positions as indicated in Figure 1a by the varying arrow 72 lengths corresponding to scattering angles, Θ1 − Θ3. Other types of Earth-orbiting satellites 73 view a given spot on the Earth from various scattering angles that vary as a function of local 74 time (e.g., geostationary) or overpass time (e.g., Sun-synchronous). When averaged over the 75 globe, the uncertainties in the anisotropy corrections are mitigated by compensation. That 76 is, any small biases at particular angles are balanced by observations taken at other angles. 77 In contrast, instruments on DSCOVR view every spot on the Earth from a single scattering 78 angle that varies slowly within a small range over the course of the Lissajous orbit. Thus, the 79 correction for anisotropy is critical. The biases in the anisotropy correction for the DSCOVR 80 scattering angle are mitigated and potentially minimized by the wide range of different scene 3 81 types viewed in a given NISTAR measurement (Su et al. 2018). 82 Su et al. (2018) described the methodology to derive the global mean daytime shortwave 83 (SW) anisotropic factors by using the CERES angular distribution models (ADMs) and a 84 cloud property composite based on lower Earth orbiting satellite imager retrievals. These 85 SW anisotropic factors were applied to EPIC broadband SW radiances, that were estimated 86 from EPIC narrowband observations based upon narrowband-to-broadband regressions, to 87 derive the global daytime SW fluxes. Daily mean EPIC and CERES SW fluxes calculated 88 using concurrent hours agree with each other to within 2%. They concluded that the SW 89 flux agreement is within the calibration and algorithm uncertainties, which indicates that 90 the method developed to calculate the global anisotropic factors from the CERES ADMs 91 is robust and that the CERES ADMs accurately account for the Earth's anisotropy in the 92 near-backscatter direction. 93 In this paper, the same global daytime mean anisotropic factors developed by Su et al. 94 (2018) are applied to the NISTAR measurements to derive the global daytime mean SW 95 and longwave (LW) fluxes. The NISTAR data and the unfiltering algorithms developed for 96 the NISTAR shortwave and near-infrared channels are detailed in section 2. The data and 97 methodology used to derive the global daytime mean anisotropic factors are presented in 98 section 3. Hourly daytime SW and LW fluxes calculated from NISTAR measurements and 99 comparisons with the CERES Synoptic flux products (SYN1deg, Doelling et al. 2013) are 100 detailed in section 4, followed by conclusions and discussions in section 5. 101 2. NISTAR observation 102 The NISTAR instrument measures Earth irradiance data for an entire hemisphere using 103 cavity electrical substitution radiometers (ESRs) and filters covering three channels: short- 104 wave (SW, 0.2-4.0 µm), near-infrared (NIR, 0.7-4.0 µm), and total (0.2-100 µm). Each 105 channel has a dedicated ESR, that by itself is sensitive to radiation from 0.2-100 µm. For 4 106 the NIR and SW channels, filters are positioned in front of each ESR to limit the incident 107 radiation to spectral bands.
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